Neutrino gravitational redshift and the electron fraction above nascent neutron stars

被引：19

作者：

Fuller, GM ^{[1
]}

Qian, YZ ^{[1
]}

机构：

[1] CALTECH,DEPT PHYS,PASADENA,CA 91125

来源：

NUCLEAR PHYSICS A | 1996年 / 606卷 / 1-2期

基金：

美国国家科学基金会; 美国国家航空航天局;

关键词：

D O I：

10.1016/0375-9474(96)00268-0

中图分类号：

O57 [原子核物理学、高能物理学];

学科分类号：

070202 ;

摘要：

Neutrinos emitted from near the surface of the hot proto-neutron star produced by a supernova explosion may be subject to significant gravitational redshift at late times. Electron antineutrinos (<(nu)over bar (e)>) decouple deeper in the gravitational potential well of the neutron star than do the electron neutrinos (nu(e), so that the <(nu)over bar (e)> experience a larger redshift effect than do the nu(e). We show how this differential redshift can increase the electron fraction Y-e in the neutrino-heated ejecta from the neutron star. Any r-process nucleosynthesis originating in the neutrino-heated ejecta would require a low Y-e, implying that the differential redshift effect cannot be too large. In rum, this effect may allow nucleosynthesis to probe the nuclear equation of state parameters which set the neutron star radius and surface density scale height at times of order t(pb) approximate to 10 s to 25 s after core bounce.

引用

页码：167 / 172

页数：6

共 7 条

[1] A NOVEL MECHANISM FOR KAON CONDENSATION IN NEUTRON-STAR MATTER [J].